Status reports of intensive programs I. Cosmology with High-Redhisft - PowerPoint PPT Presentation

@Subaru UM Jan.2007 Status reports of intensive programs I. Cosmology with High-Redhisft Type Ia Supernovae S02B-I04 02B 10 nights II. Dark Energy Measurements using SNIa in Elliptical Galaxies S05B-137 05B 5 nights 06A 5 nights S06B-085 06B 2 nights 07A 2 nights Mamoru Doi (PI) University of Tokyo

Co-investigators S02B-I04 Mamoru Doi 1 , Naoki Yasuda 2 , Nobunari Kashikawa 2 , Kentaro Motohara 1 , Tomoki Morokuma 1 , H.Furusawa 2 , K.Aoki 2 , Y.Ohyama 2 , K.Nomoto 1 , Saul Perlmutter 3 , Isobel Hook 4 , Reynald Pain 5 , Christpher Lidman 6 , Ariel Goobar 7 SXDS Team Suprime-Cam Group Supernova Cosmology Project Team 1 Univ. of Tokyo, 2 NAOJ, 3 LBNL, 4 Oxford Univ., 5 LPNHE, 6 ESO, 7 Univ. of Stochholm S05B-137, S06B-085 Mamoru Doi 1 , Naoki Yasuda 2 , Tomonori Totani 3 , Nobunari Kashikawa 2 , Kentaro Motohara 1 , Tomoki Morokuma 1 , Naohiro Takanashi 1 , Koichi Tokita 1 , Takashi Ihara 1 , H.Furusawa 2 , K.Aoki 2 , Y.Ohyama 2 , Saul Perlmutter 4 , Greg Aldering 4 , Christpher Lidman 5 , Ariel Goobar 6 SXDF Team Supernova Cosmology Project Team 1 Univ. of Tokyo, 2 NAOJ, 3 Kyoto Univ., 4 LBNL, 5 ESO, 6 Univ. of Stochholm

I Measuring Expansion of the Universe with SNIa Constant expansion “Empty” universe Deceleration Ω M , Ω R Acceleration Ω Λ

Results from “Standard Lod” measurements CMB and SDSS galaxy survey Tegmark et al. 2006 Dark Energy 75% Matter 25% Flat Universe (1 st year results) Ω Λ ( 3 r d y e a r r e s u l t s ) Ω M

Ω Λ (Dark Energy) A big mystery even for Physics d e n s i t y ρ∝a - 3 ( 1 + w ) Matter w=0 Radiation w=1/3 cosmological constant: w = - 1 w = p/ ρ = -1 : energy with “negative pressure” Energy - ∆ E ＝ ∆ V ・ p pressure p ∆ V Deceleration Parameter = ½( Ω M -2 Ω Λ +2 Ω R ） ρ Λ ~ 7×10 -30 g/cm3 → very small to measure at laboratory

Measurements with SN Redshift and Distance a ∝ (1+z) -1 slope Ｈ ０ spectroscopy present time (time) = (distance)/c Flux photometry

Type Ia Supernova • Standard Candle （ Luminosity~constant ） → WD （ @binary system ） reached Chandrasekar limit （ ~1.4solar mass ） Core collapse SNe Type II, Ib, Ic ⇔ • Large Luminosity (~whole galaxy) → measurable at cosmological distance ~15% rms By Takanashi,N.

Recent Results from SNe (Spergel et al. 2006) Ω Λ ～ 0.7 Ω M ～ 0.3 CFHT MEGACAM & HST&previous data 8-10m telescopes for spectroscopy Riess et al. 2004 Riess et al. 2006 Astier et al. 2005

II. S02B-I04 (10 nights in 2002B) S u p r i m e - C a m ： T h e m o s t p o w e r f u l i m a g e r t o f i n d d i s t a n t S N e ~ 2 0 t i m e s m o r e e f f e c t i v e t h a n A C S @ H S T F i e l d o f V i e w : x 1 0 0 i n t e g r a t i o n t i m e : ×1/5 (Yasuda et al. 2004, AAS) FoV of ACS/HST

Schedules changed original plan: FOCAS 4 nights , CISCO 6 nights, Suprime-Cam 13 nights from SXDS, 2 nights from SN ( ← ToO) bad weather for Suprime-Cam search FOCAS 2 nights → Suprime-Cam 2 nights telescope actuator trouble FOCAS 1 night → CISCO 1 night CISCO troubles, Strong Astigmatism, etc. CISCO 4 nights → Suprime-Cam 2 nights filter trouble with Suprime-Cam … real schedule: FOCAS 1 night, CISCO 3? nights, Suprime-Cam 13 nights from SXDS, 6 nights from SN → optimized for light curve observations with Suprime-Cam high quality measurements at z~1.2 ⇔

z=0.926 z=0.66 z=??? z=1.478 z=1.16? z=??? z=0.505 z=1.3? z=1.085 z=0.92 z=??? z=0.623 z=??? z=??? z=0.606 z=??? z=??? z=1.272 z=1.03 z=0.823 z=??? z=1.181 z=0.928 z=0.69 z=??? z=??? z=0.59 z=???

SN+host at z=1.28 red FOCAS （ 7200sec ） black HST/ACS （ 12000sec ） consistent Ia at z=1.18 (with VLT, Lidman et al. 2004)

2002 Fall preliminary summary (spectroscopic sample) name IAUC redshift type spectroscopy HST J-band SuF02-081 - 1.45-1.48?* VLT △ SuF02-012 SN2002lc 1.3-1.5 Keck/VLT/Subaru/HST ○ NICMOS SuF02-083 - 1.272? VLT SuF02-065 SN2002ks 1.181* Ia VLT ○ ? NICMOS SuF02-007 - 1.14? VLT/Subaru SuF02-060 SN2002kr 1.063* Ia VLT/Gemini ○ NICMOS SuF02-061 - 1.08? Keck/Subaru SuF02-017 SN2002kn 1.03 Ia? Keck/Gemini/VLT △ ISAAC/CISCO SuF02-071 SN2002kp 0.928* Keck ISAAC △ SuF02-037 SN2002kv 0.926* Keck SuF02-000 SN2002ku 0.92* Keck SuF02-002 SN2002kq 0.823* VLT SuF02-021 - 0.69 Keck SuF02-055 SN2002ky 0.66 Keck SuF02-082 SN2002kx 0.623* Keck SuF02-025 SN2002km 0.606* Ia VLT SuF02-077 SN2002kw 0.59 Keck SuF02-001 SN2002ko 0.57 Ia Keck SuF02-019 SN2002kt 0.505* Keck SuF02-028 SN2002kz 0.347? VLT SuF02-059 - 0.269 Keck *: host galaxy

Ne found with Suprime-Cam Candidates Spectr. Confir HST med followup SN Ia 2001 Spring 22 8 3 1 2002 Spring 55 13 5 4 2002 Fall 44 27 5 3 Total 121 48 13 8 Supernova Cosmology Project Final analysis follow-up observations with Keck, VLT, Gemini, HST On going

However, unexpectedly, HST ACS PSF (x, y, color, time) was not stable • Changes with • CCD (x, y) • SN Phase • Day / Night • Distortion(t) • + CTE By Naotaka Suzuki (LBNL) -4% +4% PSF Photometry

HST ACS Time Dependent Distortion

HST ACS: 2 Gyro Rotated Field

SN Ia Light Curves still to be worked out

A Survey for Faint Optical Variables By Morokuma et al. (2007) → poster First statistical results SXDF deep photometry bright Optical variability X-ray data from Newton MIR data from Spitzer HST 10 － 20 objects ★ SXDF (this work) ~1100objects faint narrow wide

Variable objects found in multi-epoch imaging of Suprime-Cam poster Morokuma et al. 2006 Variable component only → First statistical results of optical faint variables • Low-luminosity AGN population not found with deep X-ray survey • Possible most distant RR-Lyrae in our Galaxy Basic Data for future surveys • SN rate studies

Publications, plans IAUC7649 Doi et al. 2001 (7SNe), IAUC7971 Yasuda et al. (6SNe), IAUC8119 Doi et al. 2003 (13SNe) AAS Yasuda et al. 2004 Lidman et al. 2005 (VLT spectroscopy) Zero point photometry with USNO 1m Yasuda et al. 2007 (Suprime-Cam) After final HST photometry Suzuki,N.? et al. 2007 (HST) Morokuma et al. 2007a,b,.. (variability, AGN, ..) Subaru Oda et al. 2007? (SN rate) (Also contributed SXDS) AAS 2007 Becker et al. Future further usage SN cosmology only using SDSS band data Suprime-Cam, SNLS, SDSS

III. SNIa on elliptical host galaxies High-z Cluster surveys by SCP (2005-2006) HST imaging (S.Perlmutter et al) 219 orbits Subaru spectroscopy (M.Doi et al.) 14 nights VLT spectroscopy (C.Lidman et al.) 16 hours+DDT Keck spectroscopy (S.Perlmutter et al.) 6 nights+ with cluster search/study teams RCS (Gladders, Yee et al.) RDCS (Rosati et al.) IRAC (Eisenhardt et al.) XMM (Mullis et al.) RDCS 1252.9 @ z=1.23 (ISAAC and ACS)

Host extinction Sullivan et al. 2003 Host galaxy morphology of SNe with HST blue ： late type red ： E/S0 E/S0 σ =0.16 mag ⇔ All sample σ ~0.5 mag

SNe found Redshift successfully determined so far total 23 SNe Subaru 19 SNe

Preliminary SN Light curves Tomo z=1.41 J Maggie z=1.31 J z z i Midge z=0.98 Shaya z=1.35 J z z i i

Example spectra with FOCAS z=1.3 z=0.851 Spectroscopy of SN with good Light Curves total 18 Sne Subaru 12 SNe

LGAO for distant SNe KeckII+NIRC2+LGAO Submitted,2006/09 Found with HST/ACS Spectroscopy with Subaru/FOCAS

Keck+LGAO+NIRC2 H=23.9±0.14mag Exposure time 3600sec PSF(FWHM) 0.053 arcsec Pretty good accuracy

Young power See Posters Tomoki Morokuma (UTokyo, D3) SN faint spectroscopy, variability Naohiro Takanashi (UTokyo, D2) fitting SN light curve Takeshi Oda (KyotoU, D2) comparing SN rate with models Kohichi Tokita (UTokyo, D1) fitting SN spectra Yutaka Ihara (UTokyo, M2) studying SN progenitor Kohki Konishi (UTokyo, M2) studying SNIa spectral evolution …. (with SDSS SN follow-up programs etc.)

Least χ 2 fitting of Spectra (by K.Tokita) SuF02-007 SuF02-065 Flux Flux Ia t=Max z=1.156 Ia t=-1day z=1.166 6000 7000 8000 9000 6000 7000 8000 9000 S02-002 S02-002 Flux Flux Ic t=-3day z=1.084 Ia t=7day z=1.032 6000 7000 8000 9000 6000 7000 8000 9000 X axis : observed wavelength (A) Y axis : Flux (erg/sec/cm 2 /A)